Dust grain growth in ρ-Ophiuchi protoplanetary disks

By L. Ricci, L. Testi, A. Natta, K. Brooks. 2010

136 citations recorded by the source corpus.

We present new ATCA observations at 3.3 mm of 27 young stellar objects in the ρ-Oph young cluster. 25 of these sources have been detected. We analyze the sub-millimeter and millimeter SED for a subsample of 17 isolated class II protoplanetary disks and derive constraints on the grain growth and total dust mass in the disk outer regions. All the disks in our sample show a mm slope of the SED which is significantly shallower than the one observed for the ISM at these long wavelengths. This indicates that 1) class II disks in Ophiuchus host grains grown to mm/cm-sizes in their outer regions; 2) formation of mm/cm-sized pebbles is a fast process and 3) a mechanism halting or slowing down the inward radial drift of solid particles is required to explain the data. These findings are consistent with previous results in other star forming regions. We compare the dust properties of this sample with those of a uniformly selected sample in Taurus-Auriga and find no statistical evidence of any difference in terms of grain growth between the two regions. Finally, in our sample the mm slope of the SED is not found to correlate with indicators of grain growth to micron sizes in the surface layers of the inner disk.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/eed7d919f72c5c246208111f841960c8a69ba71e

How researchers see this paper

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In Astronomy and Astrophysics

1. T. Birnstiel
2. S. Andrews
3. D. Wilner
4. Anders Johansen
5. C. Dullemond
6. Xue-Ning Bai
7. L. Testi
8. Zhaohuan Zhu

In Instrumentation

1. S. Andrews
2. T. Birnstiel
3. D. Wilner
4. Anders Johansen
5. Zhaohuan Zhu
6. Xue-Ning Bai
7. C. Dullemond
8. L. Testi

Citations in the corpus

• Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “Very-long-wavelength observations show the pres- ence of mm-sized and larger grains in PPDs (see, e.g., van Boekel et al. 2004; D’Alessio et al. 2006; Natta et al. 2007; Birnstiel et al. 2010; Ricci et al. 2010; Pérez et al. 2012).”
• Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, background): “(1) Andrews et al. (2009); (2) Ricci et al. (2010b); (3) Guilloteau et al. (2011), Kenyon & Hartmann (1995). is conservative in the sense that provides the maximum possible contamination at shorter wavelengths.”
• Trapping dust particles in the outer regions of protoplanetary disks (2011, methodology): “For this case, the under-predicted fluxes are not consistent with observational data for disk ages & 1Myr, i.e. with the mean estimated ages of PMS stars in the Taurus, Ophiucus and Orion regions.”
• The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, methodology): “This shallower dust size distribution is expected from dust growth models (Birnstiel et al. 2012) and consistent with SED constraints (D’Alessio et al. 2001) and the spectral index at millimeter/centimeter wavelengths (Ricci et al. 2010a, 2010b; Pérez et al. 2015).”
• Dust Evolution and the Formation of Planetesimals (2016, background): “The observations at several (sub-)millimeter wavelengths may give some constraints on the size distribution of dust grains (Ricci et al. 2010b).”
• MILLIMETER-WAVE POLARIZATION OF PROTOPLANETARY DISKS DUE TO DUST SCATTERING (2015, background): “…disks at millimeter wavelengths, β ≈ 0 − 1, where κdust ∝ λ−β (e.g., Beckwith & Sargent 1991; Wilner et al. 2000; Kitamura et al. 2002; Andrews & Williams 2005; Ricci et al. 2010b,a; Guilloteau et al. 2011), which suggests that dust grains are grown to millimeter in size (e.g., Miyake & Nakagawa…”